@Article{ZarkaMMLELCP:2021:RoVeSo,
               author = "Zarka, P. and Magalh{\~a}es, F. P. and Marques, M. S. and Louis, 
                         C. K. and Echer, Ezequiel and Lamy, L. and Cecconi, B. and 
                         Prang{\'e}, R.",
          affiliation = "{Sorbonne Universit{\'e}} and {Sorbonne Universit{\'e}} and 
                         {Universidade Federal do Rio Grande do Norte (UFRN)} and 
                         {Universit{\'e} de Toulouse} and {Instituto Nacional de Pesquisas 
                         Espaciais (INPE)} and {Sorbonne Universit{\'e}} and {Sorbonne 
                         Universit{\'e}} and {Sorbonne Universit{\'e}}",
                title = "Jupiter's Auroral Radio Emissions Observed by Cassini: Rotational 
                         Versus Solar Wind Control, and Components Identification",
              journal = "Journal of Geophysical Research: Space Physics",
                 year = "2021",
               volume = "126",
               number = "10",
                pages = "e2021JA029780",
                month = "Oct.",
             keywords = "2736, 2756, 2784, 7534, auroral radio emissions, Jupiter radio 
                         components, magnetospheric dynamics, rotation control, solar wind 
                         control.",
             abstract = "Reanalyzing Cassini radio observations performed during Jupiter's 
                         flyby of 20002001, we study the internal (rotational) versus 
                         external (solar wind) control of Jupiter's radio emissions, from 
                         kilometer to decameter wavelengths, and the relations between the 
                         different auroral radio components. For that purpose, we build a 
                         database of the occurrence of Jovian auroral radio components 
                         bKOM, HOM, and DAM observed by Cassini, and then 
                         frequency-longitude stacked plots of the polarized intensity of 
                         these radio components. Comparing the results obtained inbound and 
                         outbound, as a function of the Observer's or Sun's longitude, we 
                         find that HOM \& DAM are dominantly rotation-modulated (i.e., 
                         emitted from searchlight-like sources fixed in Jovian longitude), 
                         whereas bKOM is modulated more strongly by the solar wind than by 
                         the rotation (i.e., emitted from sources more active within a 
                         given Local Time sector). We propose a simple analytical 
                         description of these internal and external modulations and 
                         evaluate its main parameters (the amplitude of each control) for 
                         HOM + DAM and bKOM. Comparing Cassini and Nan{\c{c}}ay Decameter 
                         Array data, we find that HOM is primarily connected to the 
                         decameter emissions originating from the dusk sector of the Jovian 
                         magnetosphere. HOM and DAM components form a complex but stable 
                         pattern in the frequency-longitude plane. HOM also seems to be 
                         related to the lesser arcs identified by Voyager. bKOM consists of 
                         a main part above (Formula presented.) 40 kHz in antiphase with 
                         HOM occurrence, and detached patches below (Formula presented.) 80 
                         kHz in phase with HOM. The frequency-longitude patterns formed by 
                         DAM, HOM and bKOM remain to be modeled.",
                  doi = "10.1029/2021JA029780",
                  url = "http://dx.doi.org/10.1029/2021JA029780",
                 issn = "2169-9402",
             language = "en",
           targetfile = "zarka_jupiter.pdf",
        urlaccessdate = "03 maio 2024"
}